1. General Relativistic MHD Simulations of Black Hole Accretion Disks John F. Hawley University of Virginia Presented at the conference on Ultra-relativistic Jets in Astrophysics Banff, July 12, 2005

2. Collaborators and References: Jean-Pierre De Villiers (U. Calgary) Steven A. Balbus (UVa, ENS) Julian H. Krolik, Shigenobu Hirose (JHU) Charles F. Gammie (Illinois) De Villiers & Hawley 2003, ApJ, 589, 458 De Villiers, Hawley & Krolik 2003, ApJ, 599, 1238 Hirose, Krolik, De Villiers, & Hawley 2004, ApJ, 606, 1083 De Villiers, Hawley, Krolik, & Hirose 2005, ApJ, 620, 878 Krolik, Hawley, & Hirose 2005, ApJ, 622, 1008

3. Accretion questions What disk instabilities are present? What disk structures arise naturally? What are the properties of disk turbulence? Is there a dynamo? How are winds and/or jets produced? Origin of QPOs and Fe K  line What are the properties of the inner disk? How does black hole spin affect accretion? How does accretion affect the black hole?

4. Direct Numerical Simulations Long term evolution towards quasi-steady state No pre-existing large-scale magnetic field Seek evolution independent of boundary or initial conditions Self-consistent evolution of disk Accretion Flows are: –Magnetohydrodynamic –Three dimensional (essential but hard!) –Dynamically unstable –Turbulent

5. Numerical Simulations Accretion Disks: Local to Global Local “Shearing boxes” Cylindrical disks (semi-global) Axisymmetric global Full 3D global simulations – Newtonian, pseudo- Newtonian Global simulations in Kerr metric

6. General Relativistic Magnetohydrodynamics Codes Wilson (1975) Koide et al. (2000) Gammie, McKinney & Toth (2003) Komissarov (2004) De Villiers & Hawley (2003) Duez et al. (2005) Fragile & Anninos Anton et al. (2005)

7. Accretion into Black Holes: GRMHD implementation Fixed Kerr Metric in spherical Boyer Lindquist coordinates Graded radial mesh - inner boundary just outside horizon;  zones concentrated at equator Induction equation of form F  + F  + F  = 0 Baryon Conservation, stress-energy conservation, entropy conservation (internal energy); no cooling First order, time-explicit, operator split finite differencing Similar to ZEUS code

8. Simulations around a Kerr hole from an Initial Magnetized Gas Torus Pressure Maximum r = 25 M Outer boundary 120M Initial poloidal field loops  Ensemble of black hole spins: a/M = 0, 0.5, 0.9, -0.9, 0.93, 0.95, 0.99, 0.998 Colors indicate density Grid resolution 192x64x192 (r,  )

9. Accretion flow structures Accretion disk Inner torus and plunging region Magnetized corona Evacuated funnel Funnel wall jet Poynting flux jet

10. Disk Evolution From r=0 to 60 M Fluid density Evolution time from t=8000 – 10000 M

11. Inner Torus Evolution From r=0 to 20 M Fluid density

12. Magnetic Field in Disk Field is tangled; toroidal component dominates Field is sub-equipartion;  Field is correlated to provide stress. Average stress values 0.1 to 0.01 thermal pressure; stress ~ ½ magnetic pressure Stress continues inside marginally stable orbit

13. Magnetic Stress vs. Novikov- Thorne Model No stress edge!

14. Angular dependence of Stress

15. Surface Density in Inner Disk a/m=0 a/m=0.5 a/m=0.9 a/m=0.998

16. Properties of the Accretion Disk Accretion disk angular momentum distribution near Keplerian After several thousand M of time, models have come into approximate steady state Disk is MHD turbulent due to the magnetorotational instability No abrupt changes at marginally stable orbit; density, velocity smooth & continuous Large scale fluctuations and low-m spiral features No stress edge; evidence for transfer of angular momentum from hole to disk Relative accretion rate drops as a function of increasing black hole spin

17. Corona formation: a/m=0.9 model Log density, azimuthal slice

18. Corona: summary Magnetic field and low density material blown up and out into a corona with mild outflow Field near equipartition on average;  varies ~ 0.1-10. Corona is bound, although less bound than original torus Large-scale motions rather than turbulence

19. What about Jets? A combination of Rotation, Accretion, Magnetic Field Young stellar objects X-ray binaries – accreting NS or BH Symbiotic stars – accreting WD Supersoft X-ray sources – accreting WD Pulsars – rotating NS AGN – accreting supermassive BH Gamma ray burst systems

20. Funnel Properties Funnel is evacuated Poloidal radial field created by ejection of field from plunging inflow into funnel Field in pressure equilibrium with corona Toroidal field can be generated by black hole spin – outgoing Poynting flux – sign of angular momentum flux same as black hole in retrograde case Unbound mass outflow at funnel wall

21. Funnel Field Formation Plot of log magnetic pressure at times 560, 640, 720, 800 M

22. Field lines and rotating Black Holes a/m = 0 a/m=0.9 a/m=0.5 a/m=.998

23. a/M = 0.9 Kerr Hole Total evolution time 10,000 M Visualization of EM Poynting flux Outer boundary of movie at r=100 M Web Page: http://www.astro.virginia.edu/VITA/jetmovie.html

24. Poynting Flux for Different Black Hole Spins

25. Funnel Wall Jet Unbound mass flux along hollow cone Accelerating force is pressure rather than magneto-centrifugal Collimation due to hot corona Mass flux increases with black hole spin: Jet flux < 1% accretion rate for a/M=0, increasing to ~10% for a/M=0.9 Funnel wall jet velocity increases with spin from 0.2c to 0.4c

26. Jet Luminosity a/M  jet  jet /  ms Poynting 0.00.0020.030.06 0.50.0130.160.34 0.90.0290.270.47 - 0.90.153.850.27 0.930.130.770.55 0.950.191.00.59 0.9980.330.560.87

27. Funnel and jets: a summary Outflow throughout funnel, but only at funnel wall is there significant mass flux Outgoing velocity ~0.4 - 0.6 c in mass flux Poynting flux dominates within funnel Jet luminosity increases with hole spin Fraction of jet luminosity in Poynting flux increases with spin Both pressure and Lorentz forces important for acceleration

28. Conclusions What disk structures arise naturally? Near-Keplerian disks, surrounded by magnetized corona What are the properties of disk turbulence? Turbulence is driven by the MRI. Highly correlated fluctuations transport angular momentum, large scale fluctuations and low-m spiral features. Toroidal fields dominate. Stress ~ ½ magnetic pressure Is there a dynamo? Yes, magnetic field is amplified and sustained at sub-thermal equipartition levels; funnel filled with large-scale radial field initially created in the plunging accretion

29. Conclusions (cont) Are winds and/or jets produced? Winds are a natural outcome (without cooling); funnel wall jet; evacuated funnel with magnetic field forms (“magnetic tower”). Poynting flux jet powered by hole spin. What are the properties of the inner disk edge? Location of inner edge time varying; physical quantities vary smoothly; stress not zero at or inside marginally stable orbit. Interaction between spinning black hole and disk. How does black hole spin affect accretion? Increasing efficiency with increasing spin. Black hole spin adds to jet power. High spin holes are being spun down. Black hole transfers angular momentum to accretion flow.